Isotopes of neon

Isotopes of neon are varieties of atoms (and nuclei ) of the chemical element of neon having different neutron contents in the nucleus. There are three stable neon nuclides : ²⁰ Ne ( isotopic abundance 90.48%), ²¹ Ne (0.27%) and ²² Ne (9.25%) ^[1] . Light ²⁰ Ne prevails everywhere.

In many alpha-active minerals, the relative content of heavy ²¹ Ne and ²² Ne is tens and hundreds of times higher than their content in air. This is due to the fact that the main mechanisms of the formation of these isotopes are nuclear reactions that occur during the bombardment of aluminum , sodium , magnesium and silicon nuclei by the decay products of heavy element nuclei. In addition, similar reactions occur in the earth's crust and atmosphere under the influence of cosmic radiation. So, for example, neutron bombardment of ²⁴ Mg and ²⁵ Mg magnesium nuclides yields ²¹ Ne and ²² Ne neon nuclides, respectively :

$\mathrm {{}_{12}^{24}Mg} +\mathrm {{}_{0}^{1}n} \rightarrow \mathrm {{}_{10}^{21}Ne} +\mathrm {{}_{2}^{4}He} .$ ${\ displaystyle \ mathrm {{} _ {12} ^ {24} Mg} + \ mathrm {{} _ {0} ^ {1} n} \ rightarrow \ mathrm {{} _ {10} ^ {21} Ne } + \ mathrm {{} _ {2} ^ {4} He}.}$ ${\ displaystyle \ mathrm {{} _ {12} ^ {24} Mg} + \ mathrm {{} _ {0} ^ {1} n} \ rightarrow \ mathrm {{} _ {10} ^ {21} Ne } + \ mathrm {{} _ {2} ^ {4} He}.}$

$\mathrm {{}_{12}^{25}Mg} +\mathrm {{}_{0}^{1}n} \rightarrow \mathrm {{}_{10}^{22}Ne} +\mathrm {{}_{2}^{4}He} .$ ${\ displaystyle \ mathrm {{} _ {12} ^ {25} Mg} + \ mathrm {{} _ {0} ^ {1} n} \ rightarrow \ mathrm {{} _ {10} ^ {22} Ne } + \ mathrm {{} _ {2} ^ {4} He}.}$ ${\ displaystyle \ mathrm {{} _ {12} ^ {25} Mg} + \ mathrm {{} _ {0} ^ {1} n} \ rightarrow \ mathrm {{} _ {10} ^ {22} Ne } + \ mathrm {{} _ {2} ^ {4} He}.}$

A number of unproductive nuclear reactions were also recorded ^[2] , in which ²¹ Ne and ²² Ne are formed - this is the capture of alpha particles by the nuclei of heavy oxygen ¹⁸ O and fluorine ¹⁹ F:

$\mathrm {{}_{8}^{18}O} +\mathrm {{}_{2}^{4}He} \rightarrow \mathrm {{}_{10}^{21}Ne} +\mathrm {{}_{0}^{1}n}$ ${\ displaystyle \ mathrm {{} _ {8} ^ {18} O} + \ mathrm {{} _ {2} ^ {4} He} \ rightarrow \ mathrm {{} _ {10} ^ {21} Ne } + \ mathrm {{} _ {0} ^ {1} n}}$ ${\ mathrm {{} _ {{8}} ^ {{18}} O}} + {\ mathrm {{} _ {{2}} ^ {{4}} He}} \ rightarrow {\ mathrm {{ } _ {{10}} ^ {{21}} Ne}} + {\ mathrm {{} _ {{0}} ^ {{1}} n}}$

$\mathrm {{}_{9}^{19}F} +\mathrm {{}_{2}^{4}He} \rightarrow \mathrm {{}_{10}^{22}Ne} +\mathrm {{}_{1}^{1}H}$ ${\ displaystyle \ mathrm {{} _ {9} ^ {19} F} + \ mathrm {{} _ {2} ^ {4} He} \ rightarrow \ mathrm {{} _ {10} ^ {22} Ne } + \ mathrm {{} _ {1} ^ {1} H}}$ ${\ mathrm {{} _ {{9}} ^ {{19}} F}} + {\ mathrm {{} _ {{2}} ^ {{4}} He}} \ rightarrow {\ mathrm {{ } _ {{10}} ^ {{22}} Ne}} + {\ mathrm {{} _ {{1}} ^ {{1}} H}}$

The source of the ²⁰ Ne light nuclide prevailing on Earth has not yet been established.

It is believed that in outer space neon is also predominantly represented by the light nuclide ²⁰ Ne. Many ²¹ Ne and ²² Ne are found in meteorites, but these nuclides are supposedly formed in the meteorites themselves under the influence of cosmic rays during wanderings in the Universe.

In addition to the three stable neon nuclides, at least sixteen more unstable are known.

Neon Isotope Table

Symbol nuclide	Z ( p )	N ( n )	Isotope mass ^[3] ( a.m. )	Excess Weight ^[3] ( keV )	Period half-life ^[4] (T _1/2 )	Spin and Parity kernels ^[4]	Prevalence isotope in nature ^[4] (%)
¹⁶ Ne	ten	6	16,025761 (22)	23996 (20)	9 zs	0 ⁺
¹⁷ Ne	ten	7	17,017672 (29)	16461 (27)	109.2 (6) ms	1/2 ^-
¹⁸ Ne	ten	eight	18,0057082 (3)	5317.17 (28)	1,672 (8) s	0 ⁺
¹⁹ Ne	ten	9	19,0018802 (3)	1751.44 (29)	17,296 (5) s	1/2 ⁺
²⁰ Ne	ten	ten	19,9924401754 (19)	-7041.9313 (18)	stable	0 ⁺	90.48 (3)
²¹ Ne	ten	eleven	20,99384668 (4)	-5731.78 (4)	stable	3/2 ⁺	0.27 (1)
²² Ne	ten	12	21,991385114 (19)	-8024,715 (18)	stable	0 ⁺	9.25 (3)
²³ Ne	ten	13	22,99446690 (11)	-5154.05 (10)	37.24 (12) s	5/2 ⁺
²⁴ Ne	ten	14	23,9936108 (4)	-5951.5 (4)	3.38 (2) min	0 ⁺
²⁵ Ne	ten	15	24,997737 (28)	-2108 (26)	602 (8) ms	(3/2) ⁺
²⁶ Ne	ten	sixteen	26,000461 (29)	430 (27)	197 (1) ms	0 ⁺
²⁷ Ne	ten	17	27,007590 (120)	7070 (110)	32 (2) ms	3/2 ⁺ #
²⁸ Ne	ten	18	28,012070 (160)	11240 (150)	18.3 (22) ms	0 ⁺
²⁹ Ne	ten	nineteen	29,019390 (290)	18060 (270)	15.6 (5) ms	3/2 ⁺ #
³⁰ Ne	ten	20	30,024800 (610)	23100 (570)	5.8 (2) ms	0 ⁺
³¹ Ne	ten	21	31,033110 (970) #	30840 (900) #	3.4 (8) ms	7/2 ^- #
³² Ne	ten	22	32,040020 (860) #	37280 (800) #	3.5 (9) ms	0 ⁺
³³ Ne	ten	23	33,049380 (860) #	46000 (800) #	<260 ns	7/2 ^- #
³⁴ Ne	ten	24	34.057030 (870) #	53120 (810) #	1 # ms	0 ⁺

Explanations for the table

The prevalence of isotopes is given for the Earth's atmosphere. For other sources, the values can vary greatly.

The values marked with a lattice (#) were not obtained from experimental data alone, but (at least partially) were estimated from systematic trends in neighboring nuclides (with the same Z and N ratios). Uncertainly determined values of the spin and / or its parity are enclosed in brackets.

The error is given as a number in brackets, expressed in units of the last significant digit, means one standard deviation (with the exception of the prevalence and standard atomic mass of the isotope according to IUPAC , for which a more complex error determination is used). Examples: 29770.6 (5) means 29770.6 ± 0.5; 21.48 (15) means 21.48 ± 0.15; −2200.2 (18) means −2200.2 ± 1.8.

Notes

↑ Isotopes of neon . www.webelements.com. Date of treatment July 8, 2009.
↑ Finkelstein D.N. Chapter IV Inert gases on Earth and in space // Inert gases . - Ed. 2nd. - M .: Nauka, 1979.- S. 83 .-- 200 p. - (“Science and technological progress”). - 19,000 copies. Archived on September 5, 2012.
↑ ¹ ² Data are given for Audi G. , Wapstra AH , Thibault C. The AME2003 atomic mass evaluation (II). Tables, graphs, and references (Eng.) // Nuclear Physics A. - 2003. - Vol. 729 . - P. 337–676 . - DOI : 10.1016 / j.nuclphysa.2003.11.003 . - .
↑ ¹ ² ³ Data are given for Audi G. , Bersillon O. , Blachot J. , Wapstra AH The NUBASE evaluation of nuclear and decay properties // Nuclear Physics A. - 2003 .-- T. 729 . - S. 3—128 . - DOI : 10.1016 / j.nuclphysa.2003.11.001 . - .

Fluorine Isotopes Periodic Table on the Isotopes of Elements Sodium Isotopes

one
H

2
He

3
Li

four
Be

five
B

6
C

7
N

eight
O

9
F

ten
Ne

eleven
Na

12
Mg

13
Al

14
Si

15
P

sixteen
S

17
Cl

18
Ar

nineteen
K

20
Ca

21
Sc

22
Ti

23
V

24
Cr

25
Mn

26
Fe

27
Co

28
Ni

29th
Cu

thirty
Zn

31
Ga

32
Ge

33
As

34
Se

35
Br

36
Kr

37
Rb

38
Sr

39
Y

40
Zr

41
Nb

42
Mo

43
Tc

44
Ru

45
Rh

46
Pd

47
Ag

48
Cd

49
In

50
Sn

51
Sb

52
Te

53
I

54
Xe

55
Cs

56
Ba

*

72
Hf

73
Ta

74
W

75
Re

76
Os

77
Ir

78
Pt

79
Au

80
Hg

81
Tl

82
Pb

83
Bi

84
Po

85
At

86
Rn

87
Fr

88
Ra

**

104
Rf

105
Db

106
Sg

107
Bh

108
Hs

109
Mt

110
Ds

111
Rg

112
Cn

113
Nh

114
Fl

115
Mc

116
Lv

117
Ts

118
Og

*

57
La

58
Ce

59
Pr

60
Nd

61
Pm

62
Sm

63
Eu

64
Gd

65
Tb

66
Dy

67
Ho

68
Er

69
Tm

70
Yb

71
Lu

**

89
Ac

90
Th

91
Pa

92
U

93
Np

94
Pu

95
Am

96
Cm

97
Bk

98
Cf

99
Es

100
Fm

101
Md

102
No

103
Lr

[isotopes-1] Isotopes of neon . www.webelements.com. Date of treatment July 8, 2009.

[filkenstein4-2] Finkelstein D.N. Chapter IV Inert gases on Earth and in space // Inert gases . - Ed. 2nd. - M .: Nauka, 1979.- S. 83 .-- 200 p. - (“Science and technological progress”). - 19,000 copies. Archived on September 5, 2012.

[AME2003-3] ¹ ² Data are given for Audi G. , Wapstra AH , Thibault C. The AME2003 atomic mass evaluation (II). Tables, graphs, and references (Eng.) // Nuclear Physics A. - 2003. - Vol. 729 . - P. 337–676 . - DOI : 10.1016 / j.nuclphysa.2003.11.003 . - .

[Nubase2003-4] ¹ ² ³ Data are given for Audi G. , Bersillon O. , Blachot J. , Wapstra AH The NUBASE evaluation of nuclear and decay properties // Nuclear Physics A. - 2003 .-- T. 729 . - S. 3—128 . - DOI : 10.1016 / j.nuclphysa.2003.11.001 . - .

Isotopes of neon

Neon Isotope Table

Explanations for the table

Notes

More articles: